Zeta Apodis

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ζ Apodis
Apus constellation map.svg
Red circle.svg
Location of ζ Apodis (circled)
Observation data
Epoch J2000       Equinox J2000
Constellation Apus [1]
Right ascension 17h 21m 59.47769s [2]
Declination −67° 46′ 14.4084″ [2]
Apparent magnitude  (V)+4.78 [3]
Characteristics
Spectral type K2 III [4]
U−B color index +1.27 [3]
B−V color index +1.21 [3]
Astrometry
Radial velocity (Rv)+11.38±0.12 [2] km/s
Proper motion (μ)RA: −37.437 mas/yr [2]
Dec.: −7.925 mas/yr [2]
Parallax (π)11.1175±0.1047  mas [2]
Distance 293 ± 3  ly
(89.9 ± 0.8  pc)
Absolute magnitude  (MV)−0.04 [1]
Details
Mass 1.51+0.99
−0.53 [5]   M☉
Radius 18.608 [6]   R☉
Luminosity 126±8 [6]   L☉
Temperature 4,486±125 [6]   K
Metallicity [Fe/H]−0.30 [5]   dex
Other designations
ζ Aps, CPD−67 3310, FK5 3374, HD 156277, HIP 84969, HR 6417, SAO 253882 [7]
Database references
SIMBAD data

Zeta Apodis is a star in the southern constellation of Apus. Its identifier is a Bayer designation that is Latinized from ζ Apodis, and abbreviated Zet Aps or ζ Aps, respectively. The star has an apparent visual magnitude of +4.78, [3] which is bright enough to allow it to be seen with the naked eye. The distance to this star is known from parallax measurements to be around 293 light-years (90 parsecs ). [2] It is drifting further away with a heliocentric radial velocity of +11 km/s. [2]

The spectrum of Zeta Apodis matches a stellar classification of K2 III, [4] with the luminosity class of III indicating it is an evolved giant star. Zeta Apodis has roughly 1.5 times the Sun's mass, [5] and expanded to 18 times the size of the Sun. It radiates 126 times the luminosity of the Sun from its photosphere at an effective temperature of 4,486 K, [6] giving it the orange-hued glow of a K-type star. [8]

Naming

In Chinese caused by adaptation of the European southern hemisphere constellations into the Chinese system, 異雀 (Yì Què), meaning Exotic Bird , refers to an asterism consisting of ζ Apodis, ι Apodis, β Apodis, γ Apodis, δ Octantis, δ1 Apodis, η Apodis, α Apodis and ε Apodis. Consequently, ζ Apodis itself is known as 異雀一 (Yì Què yī, English: the First Star of Exotic Bird.) [9]

References

  1. 1 2 Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters, 38 (5): 331, arXiv: 1108.4971 , Bibcode:2012AstL...38..331A, doi:10.1134/S1063773712050015, S2CID   119257644.
  2. 1 2 3 4 5 6 7 8 Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv: 2208.00211 . Bibcode:2023A&A...674A...1G. doi: 10.1051/0004-6361/202243940 . S2CID   244398875. Gaia DR3 record for this source at VizieR.
  3. 1 2 3 4 Johnson, H. L.; et al. (1966), "UBVRIJKL photometry of the bright stars", Communications of the Lunar and Planetary Laboratory, 4 (99): 99, Bibcode:1966CoLPL...4...99J.
  4. 1 2 Houk, Nancy; Cowley, A. P. (1978), Michigan catalogue of two-dimensional spectral types for the HD stars, vol. 1, Ann Arbor: Dept. of Astronomy, University of Michigan, Bibcode:1975mcts.book.....H.
  5. 1 2 3 Charbonnel, C.; et al. (January 1, 2020), "Lithium in red giant stars: Constraining non-standard mixing with large surveys in the Gaia era", Astronomy and Astrophysics, 633: A34, arXiv: 1910.12732 , Bibcode:2020A&A...633A..34C, doi:10.1051/0004-6361/201936360, ISSN   0004-6361
  6. 1 2 3 4 McDonald, I.; Zijlstra, A. A.; Watson, R. A. (2017-10-01), "Fundamental parameters and infrared excesses of Tycho-Gaia stars", Monthly Notices of the Royal Astronomical Society, 471 (1): 770–791, arXiv: 1706.02208 , doi: 10.1093/mnras/stx1433 , ISSN   0035-8711 Zeta Apodis' database entry at VizieR.
  7. ↑ "zet Aps". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2012-02-04.
  8. ↑ "The Colour of Stars", Australia Telescope, Outreach and Education, Commonwealth Scientific and Industrial Research Organisation, December 21, 2004, archived from the original on 2013-12-03, retrieved 2012-01-16.
  9. ↑ (in Chinese) AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 7 月 29 日 Archived 2011-05-22 at the Wayback Machine
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